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\begin{enumerate}  \item Progenitor: $20\,M_\odot$ model from \cite{2015arXiv151004643S}. This model is publicly available from \url{http://www.ucolick.org/~sukhbold/#iii}, and as stated on this website, will be available from ApJ after publication. This openly available, up to date progenitor model is ideal for this study.  \item Equation of state: The SFHo nuclear equation of state from Mattias Hempel et al. available from \url{http://phys-merger.physik.unibas.ch/~hempel/eos.html} or \url{http://www.stellarcollapse.org/equationofstate}. This EOS extends down to densities of $1\,\mathrm{g}\,\mathrm{cm}^3$. In this EOS, NSE is assumed down to these densities (which is incorrect for supernovae). However, to eliminate (for now) issues related to low density equations of state and nuclear reaction networks, this study will use only the SFHo equation of state for all densities, temperatures, and ye's.  \item Boundary and Boundary Conditions: The SFHo EOS only goes down to $0.1\,$MeV, therefore the outer boundary must be closer than $1.2\times 10^9\,\mathrm{cm}$. For this comparison, we would like the outer boundary to be taken as $10^9\,\methrm{cm}$. $10^9\,\mathrm{cm}$.  For the boundary conditions, fix the density and velocity so as to maintain a constant mass accretion rate. This is not the most physical boundary condition, but ensures the same condition is used by different groups. \section{Results}